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Discovery of a Low-Mass Companion to a Metal-Rich F Star with the Marvels Pilot Project

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Discovery of a Low-Mass Companion to a Metal-Rich F Star with the Marvels Pilot Project The Astrophysical Journal, 718:1186–1199, 2010 August 1 doi:10.1088/0004-637X/718/2/1186 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DISCOVERY OF A LOW-MASS COMPANION TO A METAL-RICH F STAR WITH THE MARVELS PILOT PROJECT Scott W. Fleming1,JianGe1, Suvrath Mahadevan1,2,3, Brian Lee1, Jason D. Eastman4, Robert J. Siverd4, B. Scott Gaudi4, Andrzej Niedzielski5, Thirupathi Sivarani6, Keivan G. Stassun7,8, Alex Wolszczan2,3, Rory Barnes9, Bruce Gary7, Duy Cuong Nguyen1, Robert C. Morehead1, Xiaoke Wan1, Bo Zhao1, Jian Liu1, Pengcheng Guo1, Stephen R. Kane1,10, Julian C. van Eyken1,10, Nathan M. De Lee1, Justin R. Crepp1,11, Alaina C. Shelden1,12, Chris Laws9, John P. Wisniewski9, Donald P. Schneider2,3, Joshua Pepper7, Stephanie A. Snedden12, Kaike Pan12, Dmitry Bizyaev12, Howard Brewington12, Olena Malanushenko12, Viktor Malanushenko12, Daniel Oravetz12, Audrey Simmons12, and Shannon Watters12,13 1 Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 326711-2055, USA; scfl[email protected]fl.edu 2 Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA 3 Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, University Park, PA 16802, USA 4 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 5 Torun´ Center for Astronomy, Nicolaus Copernicus University, ul. Gagarina 11, 87-100, Torun,´ Poland 6 Indian Institute of Astrophysics, Bangalore 560034, India 7 Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA 8 Department of Physics, Fisk University, 1000 17th Ave. N., Nashville, TN 37208, USA 9 Department of Astronomy, University of Washington, P.O. Box 351580, Seattle, WA 98195, USA 10 NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA 11 Department of Astronomy, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA 12 Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349-0059, USA 13 Institute for Astronomy, 34 Ohia Ku St., Pukalani, HI 96768-8288, USA Received 2010 April 26; accepted 2010 June 8; published 2010 July 13 ABSTRACT We report the discovery of a low-mass companion orbiting the metal-rich, main sequence F star TYC 2949-00557-1 during the Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS) pilot project. The host star has an effective temperature Teff = 6135 ± 40 K, logg = 4.4 ± 0.1, and [Fe/H] = 0.32 ± 0.01, indicating a mass of M = 1.25 ± 0.09 M and R = 1.15 ± 0.15 R. The companion has an orbital period of 5.69449 ± 0.00023 days and straddles the hydrogen burning limit with a minimum mass of 64 MJ, and thus may be an example of the rare class of brown dwarfs orbiting at distances comparable to those of “Hot Jupiters.” We present relative photometry that demonstrates that the host star is photometrically stable at the few millimagnitude level on time scales of hours to years, and rules out transits for a companion of radius 0.8 RJ at the 95% confidence level. Tidal analysis of the system suggests that the star and companion are likely in a double synchronous state where both rotational and orbital synchronization have been achieved. This is the first low-mass companion detected with a multi-object, dispersed, fixed-delay interferometer. Key words: brown dwarfs – planetary systems – stars: low-mass Online-only material: color figures 1. INTRODUCTION (12 MJ m sin i 80 MJ ) at separations of a 5AU, relative to more massive stellar companions and less massive Studies of the frequency, parameter distributions, and corre- planetary companions (Marcy & Butler 2000). Note that we lations of extrasolar planets require homogeneous samples of denote i as the inclination angle between the companion’s hundreds of planets to obtain statistically significant results. orbital angular momentum vector and the line of sight, and Moreover, such a sample must have well-understood complete- we reserve I as the inclination angle of the stellar rotation ness limits, selection effects, and biases, which are easiest to ob- axis to the line of sight. While the frequency of brown dwarf tain from a single, large-scale survey. Given current constraints companions at larger separations is still relatively uncertain on the frequency of giant planets, detection of such a large sam- (e.g., Metchev & Hillenbrand 2009), a meta-analysis of sets of ple of planetary systems generally requires a precision radial known companions to solar-type stars by Grether & Lineweaver velocity (RV) survey of many thousands of stars. Such a survey (2006), with corrections for observational bias, confirmed the also provides a wealth of ancillary science. In particular, it is lack of brown dwarfs at close separations. These authors place exquisitely sensitive to more massive companions, and because the “driest” part of the brown dwarf desert at ∼20–50 MJ , with it targets a large and broad sample of host stars, it is naturally a frequency of companions 0.5% in this range of masses. sensitive to rare binary systems in poorly explored regions of Although there has been a steady increase in the number of parameter space. known brown dwarf candidates via the RV technique (Marcy Of particular interest are the constraints on the frequency et al. 2001;Udryetal.2002; Endl et al. 2004; Patel et al. and parameter distributions of low-mass companions to solar- 2007; Wittenmyer et al. 2009; Kane et al. 2009; Jenkins et al. type stars with masses near the hydrogen burning limit. One of 2009; Niedzielski et al. 2009; Omiya et al. 2009), most of the early results from precise RV searches was the apparent these detections have been at separations a 0.8 AU. Notable paucity of brown dwarf companions with minimum masses exceptions include the transiting brown dwarf CoRoT-Exo-3b 1186 No. 2, 2010 DISCOVERY OF TYC 2949-00557-1b 1187 with a period of ∼4 days orbiting an F3V star (Deleuil et al. Table 1 2008), and HD41004Bb with a period of ∼1 day orbiting the MPP RV Observations a M dwarf component of a K–M binary system (Santos et al. BJDTDB RV σRV 2002). Brown dwarfs at such short orbital separations are (ms−1) (ms−1) of particular interest for several reasons. First, the frequency 2454101.69079 13339 94 of such systems as a function of their physical and orbital 2454105.75520 19819 98 parameters provide diagnostics that may be able to distinguish 2454106.70228 14981 96 between the various mechanisms that have been invoked for their 2454128.62211 19018 143 formation and dynamical evolution (e.g., Armitage & Bonnell 2454128.86491 17170 91 2002; Matzner & Levin 2005). In particular, these systems offer 2454130.83623 13299 94 observational constraints on the poorly understood theory of 2454136.64529 15043 85 tidal interactions between host stars and close companions (e.g., 2454136.85894 15854 139 2454163.72245 14882 91 Mazeh 2008; Pont 2009). Second, these systems are much more 2454188.69749 21003 136 likely to transit than their longer-period counterparts, as the 2454191.68122 15421 97 transit probability is inversely proportional to orbital separation. 2454194.69216 21197 115 Transiting systems yield valuable measurements on the masses, 2454195.68446 24453 102 radii, and mean densities of brown dwarfs (Stassun et al. 2006, 2454217.61115 22758 79 2007; Deleuil et al. 2008). Here we report the discovery of a candidate short-period, Note. a Errors are not scaled to account for systematics. brown dwarf companion to the metal-rich star TYC 2949- 00557-1, a main sequence F star with apparent brightness ter; previous observations with a single-object DFDI instrument ∼ V 12.1. This companion was discovered as part of the at Kitt Peak National Observatory (KPNO) resulted in the first Multi-object APO Radial Velocity Exoplanet Large-area Survey extrasolar planet discovered via this technique (Ge et al. 2006b), (MARVELS) pilot project (hereafter MPP). The MPP used the as well as the first confirmed planet via DFDI (van Eyken et al. W. M. Keck Exoplanet Tracker (Keck ET) instrument (Ge et al. 2004) and the ability to measure precise, absolute RVs with 2006a) on the Sloan Digital Sky Survey (SDSS) 2.5 m telescope DFDI (Mahadevan et al. 2008). (Gunn et al. 2006) at the Apache Point Observatory. The Keck ET instrument is a multi-object (59 targets per exposure), 2. DOPPLER OBSERVATIONS dispersed fixed-delay interferometer (DFDI; Ge et al. 2002;Ge 2002; Erskine 2002; Erskine et al. 2003). In this instrument, 2.1. MPP Observations fiber-fed starlight from the telescope is first passed through an iodine cell that acts as a stable wavelength reference. This The MPP targeted 708 F, G, and K dwarfs with 7.6 <V <12 light is then fed through a fixed-delay interferometer controlled in 12 different fields, each containing 59 stars. Data for each via a piezoelectric transducer (PZT), and finally through a field were processed simultaneously using a pipeline developed spectrograph that has a spectral resolution of R = 5100. RV for multi-object DFDI instruments (see van Eyken et al. 2004; information is then imprinted in the phases of the fringes Ge et al. 2006b; Mahadevan et al. 2008, for details of basic perpendicular to the dispersion axis of the spectrum due to a DFDI processing steps.) For each target, we determine a “quality fixed variation in the interferometer delay along this direction. factor” (QF), which we define as The primary goal of the MPP was to demonstrate a fully rms (X −X) integrated DFDI instrument capable of observing multiple stars QF = , (1) in a single exposure.
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